MPCVD法合成硼掺杂金刚石薄膜的次级发射性能

为解决电子倍增器、场发射阴极和粒子/光子探测器现有阴极材料次级发射系数低且发射不稳定的问题,对微波等离子体化学气相沉积（MicrowavePlasmaChemicalVaporDeposition,MPCVD）法结合H等离子体表面处理工艺制备的不同B₂H₆/CH₄浓度的硼掺杂金刚石薄膜的次级发射能力进行了研究。样品表面扫描电子显微镜和拉曼光谱分析结果显示,硼掺杂金刚石膜表面形貌与未掺杂的金刚石膜相似,样品表面均为高纯度的金刚石相。将置于空气中数日且未经任何表面处理的硼掺杂金刚石样品进行次级电子发射性能测试,结果显示一次电子入射能量为1keV时,得到高达18.3的二次电子发射系数。试验证实这种具有高二次电子发射系数的硼掺杂金刚石膜,暴露空气中由于表面氧化会破坏其表面的负电子亲和势,而真空中加热会使表面重新恢复负电子亲和势,这种负电子亲和势的完整保留,提高了该材料次级发射的稳定性,在器件中具有重要的应用前景。     

电子束撞击介质表面引发的带电现象分析

现有关于介质微波部件微放电的相关研究多从谐振条件及出射电子产额方面出发分析微放电发生原因及其抑制方法,而很少分析航天器表面电位对于微放电发生的影响。文章对碰撞电子与介质表面相互作用后二次电子发射特性进行综合分析;重点研究了不同介质表面初始电位情况下,恒定能量的电子束流持续轰击介质表面时介质表面电位及电子束流碰撞能量的变化趋势;并对稳定后的电子束流碰撞能量和介质表面电位进行了理论计算,计算结果表明系统平衡状态时的表面电位受初始电子能量及第二临界能量影响有明显改变。此外,文章探究了单一能量及连续能量入射介质表面时表面带电对于二次电子发射的影响,研究表明：带有电位φ的表面会使临界能量发生偏移量-eφ的相对偏移;对于连续能量的入射电子束,介质表面带电会很大程度上改变入射电子束的能量范围,从而影响微放电发生的风险。     

微型镓场发射电推力器的推力和比冲测量

电推进技术的发展推动了微推力测量技术和比冲测量技术的研究进程。为了评估已研制出的微型镓场发射电推力器的性能,进行了推力和比冲测量。研制了一种用于场发射电推力器的微推力测量平台;进行了LabVIEW开发;对测量平台进行了标定与分析,并通过试验比较了推力实测值与理论值,实测值范围为3~28μN。另外,利用飞行时间法,测得推力器在不同发射电流下的比冲数据,比冲范围为5917~8875s。     

The dynamic chromosphere: Pushing the boundaries of observations and models

The interface between the bright solar surface and the million-degree corona continues to hold the key to many unsolved problems in solar physics. Advances in instrumentation now allow us to observe the dynamic structures of the solar chromosphere down to less than $0_{.}^{″}1$ with cadences of just a few seconds and in multiple polarisation states. Such observational progress has been matched by the ever-increasing sophistication of numerical models, which have become necessary to interpret the complex observations. With an emphasis on the quiet Sun, I will review recent progress in the observation and modelling of the chromosphere. Models have come a long way from 1D static atmospheres, but their predictions still fail to reproduce several key observed features. Nevertheless, they have given us invaluable insight into the physical processes that energise the atmosphere. With more physics being added to models, the gap between predictions and observations is narrowing. With the next generation of solar observatories just around the corner, the big question is: will they close the gap?     

支板喷射超声速燃烧火焰结构实验

为明晰支板喷射超声速燃烧火焰精细结构,并探索其影响因素,利用自发辐射成像技术和平面激光诱导荧光技术(PLIF)对支板喷射超声速燃烧流场进行研究。结果表明,燃烧室内形成了典型的扩散火焰,且火焰稳定在支板尾部的回流区,宽度与支板厚度处于同等量级;支板厚度和燃料喷注当量比对火焰结构有显著影响,增加支板厚度会使火焰基底变宽,火焰长度变短,有利于燃烧室内部的快速放热和缩短燃烧室长度,增加燃料喷注当量比会使火焰长度增加,燃烧强度增大。     

On the 3D structure of the nebula around η-Carinae

The asymmetric shape of the nebula around η-Carinae (Homunculus) can be explained by a spherical expansion in a non-homogeneous medium. Two models are analyzed: an exponential and an inverse power law dependence for the density as a function of distance from the equatorial plane. The presence of a medium with variable density along the polar direction progressively converts the original spherical shell into a bipolar nebula. In the case of the nebula around η-Carinae, we know the time elapsed since the great outburst in 1840. An exact match between observed radii and velocities can be obtained by fine tuning the parameters involved, such as initial radius, initial velocity and the typical scale that characterizes the gradient in density. The observed radius and velocity of the Homunculus as a function of the polar angle in spherical coordinates can be compared with the corresponding simulated data by introducing the efficiency in a single or multiple directions. Once the 3D spatial structure of the Homunculus is obtained, we can compose the image by integrating along the line of sight. In order to simulate the observed image, we have considered a bipolar nebula with constant thickness and an optically thin emitting layer. Some simulated cuts of the relative intensity are reported and may represent a useful reference for the astronomical cuts.     

铁电阴极用于中和器研究

分析了当前小功率电推进器对零流动无推进剂阴极的需求现状。提出铁电阴极用于小功率电推进中和器的可行性。研究了厚度为0.5 mm的锆钛镧酸铅(PLZT)铁电陶瓷在低激励电压(1.0～1.2 kV)下的电子发射特性。采用单极性正高压脉冲和80 Hz重复脉冲作为激励源,在收集极获得了脉宽为320～3000 ns,最高峰值分别为34 A和27 A的发射电流。在10-5Torr的真空环境中得到了可靠的电子发射。     

An investigation of the solar cycle impact on the lower thermosphere O(S) nightglow emission as observed by WINDII/UARS

The yearly variation of the integrated emission rate of the O(¹S) nightglow in the lower thermosphere is studied and the solar cycle impact is examined from the observations of the Wind Imaging Interferometer (WINDII) operated on the Upper Atmosphere Research Satellite (UARS). More than 300,000 volume emission rate profiles of the O(¹S) nightglow observed by WINDII for 40°S–40°N latitudes during November 1991–August 1997 over half of a solar cycle are utilized. These profiles are vertically integrated for the altitude range of 80–100 km and the equivalent column integrated emission rates are then zonally averaged for bins with 10° latitude and 3 month intervals. It is found that for each latitude the O(¹S) nightglow emission rate appears to increase with increasing solar F10.7 cm flux, following a linear relationship. This characterizes the solar cycle impact on the O(¹S) nightglow, while the solar influence is modulated by a seasonal variation. Based on these variations, an empirical formula is derived for predicting the three-month averages of the O(¹S) nightglow integrated emission rate. The standard error of the estimated values from the formula is smaller than 30 Rayleigh.     

The Milky Way 3-Helium Abundance

We are making precise determinations of the abundance of the light isotope of helium, ³He. The ³He abundance in Milky Way sources impacts stellar evolution, chemical evolution, and cosmology. The abundance of ³He is derived from measurements of the hyperfine transition of ³He⁺ which has a rest wavelength of 3.46 cm (8.665 GHz). As with all the light elements, the present interstellar ³He abundance results from a combination of Big Bang Nucleosynthesis (BBNS) and stellar nucleosynthesis. We are measuring the ³He abundance in Milky Way H ii regions and planetary nebulae (PNe). The source sample is currently comprised of 60 H ii regions and 12 PNe. H ii regions are examples of zero-age objects that are young relative to the age of the Galaxy. Therefore their abundances chronicle the results of billions of years of Galactic chemical evolution. PNe probe material that has been ejected from low-mass (M≤ 2M _⊙) to intermediate-mass (M∼2–5M _⊙) stars to be further processed by future stellar generations. Because the Milky Way ISM is optically thin at centimeter wavelengths, our source sample probes a larger volume of the Galactic disk than does any other light element tracer of Galactic chemical evolution. The sources in our sample possess a wide range of physical properties (including object type, size, temperature, excitation, etc.). The ³He abundances we derive have led to what has been called “The ³He Problem”.     

航空衍生工业燃气轮机双燃料贫燃预混低污染燃烧技术

论述了航空衍生燃气轮机双燃料低污染燃烧技术的研发过程,总结了所采用的促使该技术成功发展的重要技术要点,对双燃料燃烧室可以工作的燃料-空气比的范围、燃料-空气比对CO和NOx排放的影响及过渡工况设计给予了论述,并全面总结了双燃料低污染燃烧室设计上的考虑因素.通过对多种贫燃预混的双燃料-空气模的研究设计以及长期地、持续地进行研发及燃烧试验,结果表明:设计的双燃料燃烧室在50%~100%工况范围每一点都可满足低污染要求.所研发的低污染燃烧技术以及过渡工况的设计都切实可行,可以直接用于航空发动机型号产品.